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ITC, Sensitivity and Overheads

The Integration Time Calculator (ITC) can be used to determine limiting magnitudes, exposure times, S/N ratios, background levels, etc. for a wide range of source properties, observing conditions, filters, and GMOS configurations. The ITC was used to generate tables of sensitivity estimates for imaging and spectroscopy modes. The R831 grating is not included in these example sensitivity estimates but is available for science use and is included in the ITC.


Nod and Shuffle

The GMOS Nod & Shuffle mode applies techniques adopted for the infrared to optical MOS, long-slit, and IFU (Gemini-South only) spectroscopy whereby the sky is sampled with the same pixels used to observe the science target.

The advantages of observing with Nod & Shuffle include:

  • Improved sky subtraction
  • Potential increased density of slits

Disadvantages of observing with Nod & Shuffle include:

Optomechanical Layout


The optomechanical layout of the NIFS light path:



The primary reference documents for citations to the performance and design of FLAMINGOS-2 will be found here. Until then, please cite:

"FLAMINGOS-2: the facility near-infrared wide-field imager and multi-object spectrograph for Gemini", S. Eikenberry, R. Elston, S. N. Raines, J. Julian, R. Corley, K. Hanna, D. Hon, R. Julian, D. Rashkin, B. Leckie, W. R. Gardhouse, M. Fletcher, J. Dunn, & R. Wooff, 2004 SPIE 5492, 1196

Guiding Options

TEXES has no on-instrument wavefront sensor, and PWFS2 is routinely used for all observations. As the TEXES field of view is small guide stars can be selected down to a radius of 4.3 arc-minutes.